welcome & alma project report

Welcome & ALMA Project Report

Satoru Iguchi26 December 2017

National Astronomical Observatory of Japan

Science Papers – Output Rate2

CHILE | S. I. | 26 Dec. 2017 NAOJ Project Week

ALMA Project Report

3


ALMA Status – Summary 1

Construction Project ended in Sep. 2014 (there are still a number of remaining construction items to be finished, e.g. the Residencia, which was fully completed in 2017)

4


ALMA Status – Summary 2 5


Availability of Array Elements (October 2016 to September 2017)

6


Presenter

Presentation Notes

The thick line shows the ALMA result. Dotted lines indicate space-based facilities, solid lines ground-based facilities. The dot shows the predicted number of publications at the end of the year using the publication rate of the current year for the extrapolation. The black dashed line shows the prediction of the number of publications by assuming the evolution of the Cycle 0 publications with time and convolving this with the number of accepted proposals in later cycles. The final curve is then normalized to match the publication number of the last full year.

ALMA Capabilities from Cycle 0 to 5

0

30

15

45

Cycle 0(~600 h)Sep. 2011

0.02

0.5

1

5

10

16

Base

lines

(in

km)

o Both single field interferometry and pointed mosaics

o Up to four simultaneous spectral windows available with same bandwidth and resolution

60 Band 3: 3 mm (84-116 GHz)

Band 6: 1 mm (211-275 GHz)Band 7: 850 μm (275-370 GHz)

Band 9: 450 μm (602-720 GHz)

Min

imum

Num

ber o

f Ant

enna

s

7



0

30

15

45

Cycle 1(800 h)Jan. 2013

0.02

0.5

1

5

10

16

Base

lines

(in

km)

Min

imum

Num

ber o

f Ant

enna

s

o Both single field interferometry and mosaics

o Mixed correlator modes (both high and low frequency resolution in the same observation)

60 Band 3: 3 mm (84-116 GHz)

Band 6: 1 mm (211-275 GHz)Band 7: 850 μm (275-370 GHz)

Band 9: 450 μm (602-720 GHz)

8



0

30

15

45

Cycle 2(2000 h)June 2014

0.02

0.5

1

5

10

16

Base

lines

(in

km)

Band 3: 3 mm (84-116 GHz)Band 4: 2 mm (125-163 GHz) Band 6: 1 mm (211-275 GHz)Band 7: 850 μm (275-370 GHz)Band 8: 650 μm (385-500 GHz) Band 9: 450 μm (602-720 GHz)

Min

imum

Num

ber o

f Ant

enna

s

o Both single field interferometry and mosaicso Spectral-line observations with all Arrays and

continuum observations with the 12-m Array and the 7-m Array.

o Polarization (on-axis, continuum, selected frequencies in Band 3, 6 and 7, no ACA, no mosaics)

o Mixed correlator modes (both high and low frequency resolution in the same observation)

60

9



0

30

15

45

Cycle 3(2100 h)Oct. 2015

0.02

0.5

1

5

10

16

Base

lines

(in

km)

Min

imum

Num

ber o

f Ant

enna

s

o High-fidelity imaging, mosaickingo Flexible correlator (up to 16

narrow spectral windows, or 8 GHz bandwidth)

o Polarization (linear polarization in continuum and spectral line)

60 Band 3: 3 mm (84-116 GHz)Band 4: 2 mm (125-163 GHz) Band 6: 1 mm (211-275 GHz)Band 7: 850 μm (275-370 GHz)Band 8: 650 μm (385-500 GHz) Band 9: 450 μm (602-720 GHz) ) Band 10: 350 μm (787-950 GHz)

10



0

30

60

15

45

Cycle 4(3000 h)Oct. 2016

0.02

0.5

1

5

10

16

Base

lines

(in

km)

Min

imum

Num

ber o

f Ant

enna

s

Band 3: 3 mm (84-116 GHz)Band 4: 2 mm (125-163 GHz) Band 6: 1 mm (211-275 GHz)Band 7: 850 μm (275-370 GHz)Band 8: 650 μm (385-500 GHz) Band 9: 450 μm (602-720 GHz) Band 10: 350 μm (787-950 GHz)

o Large programo ACA standaloneo mmVLBIo Solar Observation

11



0

30

60

15

45

Cycle 5(4000 h)Oct. 2017

0.02

0.5

1

5

10

16

Base

lines

(in

km)

Min

imum

Num

ber o

f Ant

enna

s

o Maximum baseline length of 16 km at Bands 3, 4, and 6

o Band 5 at short baseline configuration only

Band 3: 3 mm (84-116 GHz)Band 4: 2 mm (125-163 GHz) Band 6: 1 mm (211-275 GHz)Band 7: 850 μm (275-370 GHz)Band 8: 650 μm (385-500 GHz) Band 9: 450 μm (602-720 GHz) ) Band 10: 350 μm (787-950 GHz) Band 5: 1.5 mm (163-211 GHz)

12


Planned ALMA Capabilities of Cycle 6

0

30

60

15

45

Cycle 6(~4300 h)Oct. 2018

0.02

0.5

1

5

10

16

Base

lines

(in

km)

Min

imum

Num

ber o

f Ant

enna

s

o Maximum baseline length of 16 km at Bands 3, 4, 5, 6, 7?

o Band 8 as a standard modeo Circular polarization (possibly)o Proposal deadline is on April 19

o APRC chair – Masao Saito

Band 3: 3 mm (84-116 GHz)Band 4: 2 mm (125-163 GHz) Band 6: 1 mm (211-275 GHz)Band 7: 850 μm (275-370 GHz)Band 8: 650 μm (385-500 GHz) Band 9: 450 μm (602-720 GHz)Band 10: 350 μm (787-950 GHz) Band 5: 1.5 mm (163-211 GHz)

13


Planned ALMA Capabilities of Cycle 7

0

30

60

15

45

Cycle 7(~4300 h)Oct. 2019

0.02

0.5

1

5

10

16

Base

lines

(in

km)

Min

imum

Num

ber o

f Ant

enna

s

o Maximum baseline length of 16 km at Bands 3, 4, 5, 6, and 7

o Circular polarization (possible for Cycle 6)o Wide-field mosaicking in polarization o Single-dish spectral line by Band 9&10o Total Power Continuumo APRC chair – Masao Saito

Band 3: 3 mm (84-116 GHz)Band 4: 2 mm (125-163 GHz) Band 6: 1 mm (211-275 GHz)Band 7: 850 μm (275-370 GHz)Band 8: 650 μm (385-500 GHz) Band 9: 450 μm (602-720 GHz)Band 10: 350 μm (787-950 GHz) Band 5: 1.5 mm (163-211 GHz)

14


ALMA Status: Receivers

Receiver Bands currently installed on all antennas,in construction and under study: Band 1: 6 mm (35-52 GHz) Band 2: 4 mm (65-90 GHz) Band 3: 3 mm (84-116 GHz) Band 4: 2 mm (125-163 GHz) Band 5: 1.5 mm (163-211 GHz) Band 6: 1 mm (211-275 GHz) Band 7: 850 μm (275-370 GHz) Band 8: 650 μm (385-500 GHz) Band 9: 450 μm (602-720 GHz) Band 10: 350 μm (787-950 GHz)

1 2

15


Steady State Operations and Beyond Performance based milestone

– 7300 hours scheduled for science activities annually• Successful hours offered ~ 4300 (85% of array elements at a given time of 5000)• ≤970 h for weather and array calibration each• ≤320 h for technical issues• Testing and further development ~730 hours

– Minimum of 56 antennas in service (daytime)• 43 12-m + 10 7-m + 3 SD

Challenges– Weather recovery; Antenna/receiver uptime (corrective maintenance)

Capability Driven Milestone– 7300 hours scheduled for science activities annually– Single Dish: continuum and high frequency– Polarization: Stokes V and wide fields– Long Baseline: Band 7 maximum baseline length

16


ALMA Status – Summary 3

Bring ALMA to Full & Stable Operations Increase the new science capabilities

• Roadmap for Future Developments in next 10-20 years that will enable ALMA to extend the frontiers of science even further

17


ALMA Upgrade Planning

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Band 1 Artificial Calibration Source

Output: three EA led projects/studies

Output: Antenna Cost vs performance

Output: Software/Calibration strategies and demands

2015Antenna Structure Development WS

2013 Development WS

2011 Development WS

2014 ASTE/ALMA Development WS

2016 Development WS

FidelityOutput: New science demands for ALMA

THz Wideband SpectrometerTES CamMulti-beam

Output: Science requirements, ASTE/ALMA dev timeline

Sensitivity Wide IFFOV

Band 11

2017Long Baseline WS(Kyoto, Oct 3-5, 2017)

Angular Res.

EA ALMA Development Workshops – Status –

http://alma-intweb.mtk.nao.ac.jp/~diono/meetings/ASTE_ALMA_2014/

http://alma-intweb.mtk.nao.ac.jp/~diono/meetings/EA_Development_Meeting/

http://alma-intweb.mtk.nao.ac.jp/~diono/meetings/NRO_ALMA_2015/

http://alma-intweb.mtk.nao.ac.jp/~diono/meetings/NRO_ALMA_2016/

http://alma-intweb.mtk.nao.ac.jp/~diono/meetings/longBL2017/

Output: AIs for long baseline testing. Need to identify solid science case.

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• Origins of Galaxies– The ability to detect spectral line emission from CO or C+ in a normal

galaxy like the Milky Way at a redshift of z = 3, in less than 24 hours of observation;

• Origins of Planets– The ability to image the gas kinematics in a solar-mass protoplanetary disk

at a distance of 150 pc, enabling one to study the physical, chemical, and magnetic field structure of the disk and to detect the tidal gaps created by planets undergoing formation;

• High-fidelity Images – The ability to provide precise images at an angular resolution of 0.1.”

First five year Science Goals of ALMA Operations

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• Organized by D. Iono

– Participants: more than 80http://alma-intweb.mtk.nao.ac.jp/~diono/meetings/longBL2017/

ALMA Long Baseline Workshop

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Wavelength [µm] Credit: AURA

Fine

r res

olut

ion

Spat

ial R

esol

utio

n[a

rcse

c]ALMA Potential Performance

/ SUBARU

/ TMT

Solid lines：under operation or terminated

Dashed lines：under construction or planning

ALMA will continue to be the forefront telescope in spatial resolution among the next generation telescopes planning in the coming 30 years.

0.01 arcsec corresponds to 1 AU at the distance of ~300 light yrswhere many protoplanetary disks are present.

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ALMA Management Structure

23


ALMA Top Management– 2017 Dec: ALMA Management Team (AMT) –

• ALMA Top Management

EA: Satoru Iguchi EU: Leonardo Testi (Interim) NA: Phil Jewell

JAO: Stuartt Corder (Acting Director)

24


Sean Dougherty

EA ALMA Support Center (EAASC)– Previous Organization Structure –

EAASC Head(S. Iguchi)

EA IET Manager

(S. Asayama)

EA ARCManager

(K. Tatematsu)

EA EPO Officer

(M. Hiramatsu)

EA ICT Manager

(G. Kosugi)

EA Development Programme

Manager(S. Asayama)

EA Project Scientist(D. Iono)


EA ALMA Support Center (EAASC)– New Organization Structure –

EAASC Head(S. Iguchi)

EA IET Manager

(S. Asayama)

EA ARCManager

(H. Nagai)

EA EPO Officer

(M. Hiramatsu)

EA ICT Manager

(G. Kosugi)

EA Development Programme

Manager(A.Gonzalez)

EA Project Scientist(D. Iono)


The Atacama Large Millimeter/submillimeter Array (ALMA), an international astronomy facility, is a partnership of ESO (representing its members states), NSF (USA) and NINS (Japan), together with

NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The

National Radio Astronomy Observatory is a facility of the National Science Foundation operated under the cooperative agreement by Associated Universities Inc. We than all those who have

contributed to making the ALMA project possible. CHILE | S. I. | 26 Dec. 2017

NAOJ Project Week

welcome & alma project report

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